BELGIAN ASTRONOMICAL SOCIETY V.V.S. - Working Group Variable Stars Cataclysmic Variables Circular No.39 1995, June 01 Ed.: T. Vanmunster, Walhostraat 1A, 3401 Landen, BELGIUM Internet: tvanmuns@innet.be TEL. 32-11-831504 P. Van Cauteren, de Borrekenslaan 54, 2630 Aartselaar, BELGIUM Internet: pvancaut@innet.be TEL. 32-3-8774098 =================================================================== The Cataclysmic Variables Alert Programme - Annual Report #1 ++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++ Precisely one year ago, we initiated the Belgian Cataclysmic Variables Alert Programme (CVAP). It is a cataclysmic variables observation project, similar to (but complementary with) the Recurrent Objects Programme of the UK-based "The Astronomer Group" (Hurst 1989). The CVAP consists of poorly observed objects, for which professional astronomers have shown interest and have requested assistance in providing a continuous monitoring. It has been complemented with objects, for which only a few historical observations exist, or for which anomalies in predicted behaviour have been detected. This report describes the first year of CVAP activity, and highlights some of the early successes achieved. Additionally, we present a num- ber of extremely interesting objects, that will be added to the CVAP. 1. CVAP activity in the period May 1994 - May 1995 -------------------------------------------------- The CVAP was officially announced in Cataclysmic Variables Circular CVC 2 (May 5, 1994). It started as a monitoring programme of 12 cata- clysmic variables, of which the identification and/or classification was uncertain or unknown. For each of these objects, Paul Van Cauteren issued a set of finding charts and a sequence based on the Guide Star Catalog GSC. Although GSC-based magnitudes sometimes tend to be inaccurate, this approach allowed us to create sequences for poorly studied objects, which otherwise probably would have remained unmonitored for several more years. The CVAP was first revised on 1994, November 1 (CVC 21). 8 more objects were added to the programme, and one variable (AR UMa) was removed. CVAP charts have been distributed to observers world-wide. We now receive regular contributions from amateurs in the US, UK, Hungary, Denmark, Germany, Japan and Belgium. Our first year of CVAP activity has been characterised by some very nice observational results. Among the most important are : IR Lyr : this object is classified as a possible UG star in Downes and Shara (1993). It has been observed, as part of the CVAP, during activity over a period of several months by 4 obser- vers. Main contributions were received from Gary Poyner (UK) and Tonny Vanmunster (B). A first interpretation of the resulting photometric light curve clearly illustrates that IR Lyr certainly does not belong to the UG-type dwarf novae, but presumably is a semi-regular or irregular type of variable. A further follow-up is required to precisely determine the variability type of this star. QY Per : discovered as an UG star by Hoffmeister (1966), this variable remained unobserved for many decades. It finally was re- covered by Tonny Vanmunster on October 25, 1994, and confirmed by Eric Broens (B) within minutes (CVC 20). These constituted the first visual observations since the discovery date. As a result of the outburst notification, Nick James (UK) was able to perform accurate astrometry on the object, which showed that it was not exactly located at the position in Downes and Shara (1993). The outburst itself was a rather short-lived one and lasted for only 3 nights, after which the variable returned to its minimum state. UW Tri : UW Tri (= Nova Tri 1983) was discovered by Kurochkin in 1983, and subsequently classified as a possible nova on the basis of its light curve. The 1983 outburst lasted at least 32 days. UW Tri was recovered in outburst on March 3, 1995 by Tonny Vanmunster (CVC 29) and confirmed within minutes by Eric Broens and Gary Poyner. Nick James obtained a CCD image of UW Tri and calculated a precise position for the object. Professional astronomers in the USA, UK and Japan (T. Kato and the Ouda Team) have closely monitored the 1995 outburst of UW Tri, which lasted for more than two weeks. Results are currently being processed and might allow the determination of the exact nature of this intriguing variable. 2. New additions to the CVAP ---------------------------- Table 1 lists the new CVAP programme, which includes the addition of 17 new objects. The newly selected targets (DK Cas, TX Tri, WY Tri, V336 Per, NS Per, DE Cnc, RU LMi, Leo1, T Leo, GW Lib, V699 Oph, DV Dra, V1505 Cyg, V1711 Cyg, FX Cep, V1089 Cyg, KM Lac) were added, taking into account various criteria : - for some of them no (or only one) reference in the Simbad Catalog is given, indicating that it are rather poorly studied objects, - some are not confirmed as a CV, contrary to what one might expect from the classification in Downes and Shara (1993), - for some the identification itself is still uncertain, - for many, no visual observations seem to exist, as we could derive from Vanmunster and Howell, 1995, - some are possible TOAD's (Howell 1995), and thus require detailed monitoring in case of an outburst detection. Finding charts and GSC-based sequences currently are prepared by Paul Van Cauteren, and shortly will be available to observers, upon simple request. ____________________________________________________________ | | | THE CATACLYSMIC VARIABLES ALERT PROGRAMME [CVAP] | |___________________________________________________________| VARIABLE RA DECL TYPE MAG_RANGE REMARKS NAME [2000.0] MAX MIN -------- ------------------------ ---- -------------- ------- * DK Cas 00 18 08.39 +57 26 03.2 UGSS 15.3p 19.5:p [2,3] AS Psc 01 28 10. +31 14 57. UG 16.6p 21.5:p [5,7] * TX Tri 01 37 37.31 +30 02 48.3 UGSS 14.5B 18.2B [5] TU Tri 01 39 15.39 +31 24 19.8 UG 14.8p [18.0p [5,7] * WY Tri 02 25 00.57 +32 59 54.9 UG 13.8p [17.0p [5,7] KW And 02 35 18.12 +41 14 01.6 UG 14.8p 22p [7] PU Per 02 42 16. +35 40 29. UG 14.7p 20:p [5,7] PV Per 02 42 53.57 +38 04 02.6 UG 14.9p 20:p [5,7] UW Tri 02 45 17.2 +33 31 25.5 UGWZ? 15p [21p [7] QY Per 03 15 37.93 +42 28 00.9 UG 14.2p [20p [7] * V336 Per 03 22 55. +41 37 03. UG 14.3p [20p [5,7] V701 Tau 03 44 00. +21 57 15. UG: 15.0p [21p [5,7] * NS Per 04 18 44.54 +51 07 29.6 UG 15p [18p [5,7] V650 Ori 05 31 08.25 +09 45 09.9 UG: 15.5p [17.5p [5,7] FS Aur 05 47 48.42 +28 35 10.0 UGZ: 14.4v 16.2v V421 Tau 05 48 22.98 +22 42 01.2 UG 14.5p 20p [5,7] CI Gem 06 30 05.80 +22 18 56.6 UGSU: 14.7p 18.5p [5] AQ CMi 07 14 34.84 +08 48 05.0 UG: 14.5[ [16.5p [5,7] * DE Cnc 08 35 27.33 +19 45 29.2 UG 14.6p 18.0p [5] * RU LMi 10 02 07.61 +33 50 59.3 UG 13.8p 19.5p [5,7,9] SS LMi 10 34 06.0 +31 07 59. UG/N 15p [21p [5,7] * - Leo1 11 06 40.28 +01 54 49.7 CV: 14.1B * T Leo 11 38 27.01 +03 22 07.0 UGSU 10B 15.7B [6,7] * GW Lib 15 19 55.32 -25 00 24.7 N/UG 9p 18.5p [8] * V699 Oph 16 25 22.65 -04 40 25.3 UG 13.8p 18.5p [5,10] * DV Dra 18 17 24.98 +50 48 14.5 UGWZ? 15.0B [21p [5,7] IR Lyr 18 23 53.62 +39 18 58.9 ? 14.6p 16.0p V358 Lyr 18 59 34. +42 24 14. UGWZ? 16p [20p [5,7] * V1505 Cyg 19 29 49. +28 32 52. UGZ 15.2p [17.5p [1,3,4] V1289 Aql 19 38 42.25 +12 16 29.4 NL: 13p [15.5p [5] V337 Cyg 19 59 51. +39 13 52. UG: 14.4p [16.5p [5,7] IO Del 20 26 47. +18 30 59. UG: 15.5p [20p [5,7] * V1711 Cyg 20 55 00.70 +44 55 30.7 UG: 15.0p [17.5p [1,3,7] * FX Cep 21 03 06.19 +66 10 23.5 UGSS 15.0p 17.5p [2,3] EV Aqr 21 06 19. +00 51 53. UGZ: 12.1p [14.2p [5,7] * V1089 Cyg 21 44 18. +47 54 50. UGSS 15.0p 18.5p [2,3,4] * KM Lac 22 13 49.92 +55 28 23.6 UGSS 14.8p [17.4p [2,3,7] Table 1 : The CVAP programme (30.05.1995) [1] No references in Simbad Catalog [2] Only one reference in Simbad Catalog [3] Not confirmed as CV, contrary to what might be suspected by the classification in Downes and Shara (1993) [4] Identification uncertain [5] No visual observations listed in Vanmunster and Howell (1995) [6] See motivation in CVC 38 [7] Suspected TOAD (Howell 1995) [8] Known TOAD (Howell 1995) [9] Shows rather odd light curve (Howell et al. 1990) [10] True nature of this object unknown (Wenzel 1993) 3. The Second Year of CVAP Activity ----------------------------------- It's both hard and dangerous to make predictions on cataclysmic variables. The same holds -even more- for CV alert programmes. We nevertheless are very optimistic about the CVAP future. The recent additions to the programme clearly illustrate that we now have a very appealing monitoring programme, and the many enthusiastic reactions we received from both amateurs and professionals in recent months have stimulated us to continue our efforts. We are now starting the process of fixing objects for future inclusion in the CVAP. We hope to be able to identify a number of variables, that become brighter than magnitude 13 or so at maximum, in an attempt to make the CVAP more attractive to amateurs with small- and medium sized aperture. Suggestions would be more than welcome. Finally, we feel pretty confident that one of the highlights of the second year of CVAP activity will be the introduction of Belgian CCD work in our photometric results. We'll soon be back on this. References ---------- Downes R.A., Shara, M.M. 1993, PASP, 105, 127-245 Hoffmeister, 1966, Astron. Nachr., 289, H.3, 139 Howell et al., 1990, PASP, 102, 758 Howell, S. 1995, AJ, 439, 337-345 Hurst, G. 1989, UK Nova/Supernova Patrol, Recurrent Objects Catalogue Vanmunster and Howell, 1995, in preparation Wenzel, W. 1993, Mitt.Ver.Sterne, 12.9, 155 Tonny Vanmunster